0
Assigned ID: 583
----- Attempting Submission 1 (Fri Apr 08 16:38:34 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-1
----- Attempting Submission 2 (Fri Apr 08 17:45:06 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-2
----- Attempting Submission 3 (Fri Apr 08 19:55:16 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-3
----- Attempting Submission 4 (Fri Apr 08 23:57:07 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-4
----- Attempting Submission 5 (Sat Apr 09 00:15:05 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-5
----- Attempting Submission 6 (Sat Apr 09 00:19:29 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-6
----- Attempting Submission 7 (Sat Apr 09 00:25:26 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-7
----- Attempting Submission 8 (Sat Apr 09 01:00:26 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-8
----- Attempting Submission 9 (Sat Apr 09 01:04:09 GMT 2016) -----
HST Phase I Proposal 583 (HST_Proposal.apt) successfully submitted.
Receipt: # 583-9
RA Uncertainty is larger than expected.
DEC Uncertainty is larger than expected.
RA Uncertainty is larger than expected.
DEC Uncertainty is larger than expected.
We have added newly discovered SNe.
119762179
----- Attempting Submission 1 (Thu Jul 21 23:42:45 GMT 2016) -----
----- Attempting Submission 2 (Wed Dec 07 06:04:46 GMT 2016) -----
----- Attempting Submission 3 (Wed Jan 04 05:55:15 GMT 2017) -----
----- Attempting Submission 4 (Wed Jan 04 16:56:17 GMT 2017) -----
----- Attempting Submission 5 (Wed Jan 25 21:39:49 GMT 2017) -----
----- Attempting Submission 6 (Tue Jan 31 22:17:04 GMT 2017) -----
----- Attempting Submission 7 (Wed Feb 01 13:48:41 GMT 2017) -----
----- Attempting Submission 8 (Tue Feb 28 22:27:56 GMT 2017) -----
----- Attempting Submission 9 (Wed Mar 01 16:42:22 GMT 2017) -----
----- Attempting Submission 10 (Wed Mar 08 11:56:44 GMT 2017) -----
Our target coordinates (SNe in COSMOS and SXDS) are only known to 45 arcminutes. When we find a SN to observe, we will enter the exact coordinates.
SUbaru Supernovae with Hubble Infrared (SUSHI)
During the next two HST Cycles, the Subaru Strategic Program (SSP) will conduct a rolling search with Hyper Suprime-Cam (HSC) that will discover and study scores of very high quality SNe Ia up to redshift of ~1.5. However, above a redshift of one, the Subaru photometry will be limited to the UV and blue rest-frame of the SNe. By combining the HSC light curve with just one non-disruptive ToO observation and a "reference image" (after the SN has faded) from HST for each of 46 SNe, we will improve the dark energy Figure of Merit (FoM) obtainable from all past and present high-redshift SN searches by a factor of 2.3. This opportunity is unique. Because this search requires frequent changes of the massive HSC at the Subaru prime focus, it will not be repeated for the foreseeable future.
Investigators from this proposal will search for high-redshift supernovae using the Subaru Hyper-Suprime Cam. Twice per month (the Subaru observations are during dark and gray time), we expect to place two 1-orbit non-disruptive ToOs on the schedule (the number may be zero to three, depending on the weather). We expect almost all of these triggers will have no roll constraint (with only rare exceptions when two supernovae can be observed in one pointing but only corner-to-corner). We will know the coordinates of these ToOs to within 45 arcminutes, as only one Subaru field will be monitored at any given time. Our triggers will consist of F105W and F140W WFC3 imaging, although other filters (F125W and F160W) may be used if archival data already exists at the SN location. Approximately one year later, after the supernovae have faded, we will obtain reference (template) images of the field. There are no scheduling constraints for these images (we may have roll constraints in rare cases when two host-galaxies are observable in one pointing but only corner-to-corner).
We have experience ordering the observations in each orbit such that the F105W is in the darkest part to avoid the risk of high background from He emission (the F140W can be placed at any point in the orbit). The ground visibility and location of each field implies that there will be dark part of each orbit. We will require an uninterrupted sequence of observing to make sure that the filters occur where we expect in the orbit.
As we are using WFC3 IR to observe faint sources, we would like to avoid orbits significantly contaminated by SAA persistence.
Intergalactic Medium and Cosmology
6
false
false
false
false
false
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SUPPORTED
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
NO
J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
NO
J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
NO
J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
NO
J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
NO
J2000
EXT-STAR
SUPERNOVA
SUPERNOVA TYPE IA
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EXT-STAR
SUPERNOVA
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EXT-STAR
SUPERNOVA
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SUPERNOVA
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SUPERNOVA
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SUPERNOVA
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Imaging
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Imaging
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WFC3/IR
Imaging
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F105W
WFC3/IR
Imaging
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F140W
WFC3/IR
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F105W
WFC3/IR
Imaging
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F140W
WFC3/IR
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Imaging
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WFC3/IR
Imaging
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F105W
WFC3/IR
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WFC3/IR
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WFC3/IR
Imaging
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Imaging
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F140W
WFC3/IR
Imaging
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WFC3/IR
Imaging
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WFC3/IR
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WFC3/IR
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F140W
WFC3/IR
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F125W
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Imaging
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F160W
WFC3/IR
Imaging
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WFC3/IR
Imaging
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WFC3/IR
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F160W
WFC3/IR
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WFC3/IR
Imaging
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